[1]} examined non-relativistic radiative shocks in the disc accretion and solved analytically the structure of the radiative precursor region for both the gas
and radiation-pressure dominated cases.
Since our model Thin1 with gas-pressure dominant and optically thin matter shows almost the same result
as the adiabatic case, the radiative effects on the shock are negligible.
We compare the analytical structure of the precursor region in the pressure dominant flow
with the results by the simulations for model Thick5.
The structure equation for the radiative precursor in the radiation-pressure dominated case is given as [1]},
\({ 1 \over {\tau _{1} \beta _{1}} } \frac{\tilde{P}^2}{\tilde{\Sigma }^3} \frac{d \tilde{P} }{d x} ={1\over 2} {\gamma \over {\alpha _{1}}}M_{1}^2 ({1\over {\tilde{\Sigma }^2}}-1) + 4 ({\tilde{P}^2\over {\tilde{\Sigma }^2}} - 1),\) 
